The Cosmic γ-ray Background from supernovae

Details The Cosmic γ-ray Background from supernovae The Cosmic γ-ray Background from supernovae

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..410.1223w&link_type=abstract

The fourth compton symposium. AIP Conference Proceedings, Volume 410, pp. 1223-1227 (1997).

Computer Science

20

Supernovae, Gamma-Ray Sources, Gamma-Ray Bursts, Star Formation

Scientific paper

The Cosmic γ-ray Background (CGB) near photon energies Eγ~1 MeV may be partly, or even completely, due to γ-ray production in supernovae. In particular, γ-ray line emission from the decay chain 56Ni-->56Co-->56Fe (847, 1238, 1770, 2599, 2030, 3250 keV) is the dominant source for the SN-induced CGB. Although iron synthesis occurs in all types of supernovae, SNIa contribute predominantly to the background mostly due to higher photon escape probabilities. Estimates of the global star formation history in the local universe yield a present-day rate density of ~=3.7×10-2 h3 Msolar Mpc-3 yr-1, but the star formation rate was about ten times higher at a redshift of order unity. The rate then decreases again, reaching the present-day value near redshifts ~=5. In addition to γ-rays from SNIa we also consider contributions to the CGB due to lines from SNII (such as 26Al at 1.8 MeV, 44Ti at 1.157 MeV, and 60Co at 1.17 & 1.33 MeV). The γ-ray spectrum of Model W10HMM (Pinto & Woosley [8]) was time integrated to derive a template spectrum for Type II supernovae. For SNIa we also included the γ-ray continuum, using the W7 model (Nomoto et al. [5]), integrated over 600 days, as template. We discuss the various contributions of supernovae to the CGB, and emphasize the value of γ-ray observations in the MeV range as a potential tool for studies of cosmic chemical evolution.

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